Variability of the intrinsic polarization of the supergiant binary VV Cephei

Details Variability of the intrinsic polarization of the supergiant binary VV Cephei Variability of the intrinsic polarization of the supergiant binary VV Cephei

Aug 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987aj.....94..484p&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 94, Aug. 1987, p. 484-500.

Astronomy and Astrophysics

Astronomy

3

Binary Stars, Linear Polarization, Periodic Variations, Polarimetry, Stellar Spectrophotometry, Supergiant Stars, Circular Polarization, M Stars, O Stars, Stellar Temperature

Scientific paper

Detailed linear polarization variations in red, green, blue, and ultraviolet bandpasses have been observed for VV Cep from before primary eclipse through secondary conjunction. Polarization activity increased with decreasing wavelength and as periastron was approached. Near periastron, a large polarization pulse lasted for about 440 days. It is suggested that this pulse signaled the ejection of material from the supergiant due to the latter overfilling its Roche lobe. The mean polarization variation with Keplerian phase is reproduced by a multiparameter model of the system's scattering geometry. The model indicates that the observed intrinsic polarization is dominated by a contribution from the supergiant towards long wavelengths, while an O star disk and adjoining portions of an M star gas stream provide a polarimetric component that dominates towards shorter wavelengths. The model parameters lead to a value of 10 to the 11th/cu cm for the average electron density and roughly 10 to the -7th solar mass for the mass of the O star disk.

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